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USGS1978

Geologic map of the Amazonis Quadrangle of Mars

The Amazonis quadrangle lies within the northern sparsely cratered hemisphere of Mars ( Carr and others, 19 73) The dominant structural ad physiographic features of the quadrangle are low feature - less plains ( Amazonis Planitia) in the center third of the quadrangle, the western flanks of the large volcanic construct, Olympus Mons, and its associated aureole deposits (Lycus Sulci ), which lies on the eastern slopes of the plains, a n d in a area of rough knobby terrain along the west edge of the quadrangle. The central plains descend northward into the circumpolar lowlands (Arcadia Plan itia, Vastitas Borealis) and rise southward where they are bounded by the cratered terrains of the equatorial region of Mars.

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USGS1978

Geologic map of the Aeolis Quadrangle of Mars

Two principal physiographic provinces of Mars are represented in the Aeolis quadrangle: (1) Elysium Plan itia in the north is part of a broad planet-encircling belt of relatively young lowland plains, and (2) cratered highlands in the south consist of roughly primitive terrain that extends to polar deposits around the southern ice cap (Condit and Soderblom, 1978: Scott and Carr , 1978). These two terrains are separated by an irregular discont inuous northwest-trending scarp that becomes less conspicuous and more segmented toward the east part of the ma p area. Two large channels transect the highlands; they widen northward downslope and have other features cha racteristic of terrestrial river beds . However, now fans or deltaic forms are visible at their mouths and their floors merge with the plains. One large shield volcano, Apollinaris Patera, projects above the plains adjacent to the highlands in the northeast part of the quadrangle. More than 4 km of relief occur across the region from the high plateau in the south and west, downslope northward to plains.

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USGS1979

Geologic map of the Cebrenia quadrangle of Mars

Most of the Cebrenia quadrangle (lat 30˚ to 65˚ N., long 180˚ to 240˚ W.) is in the circumpolar plains of Mars. Craters from an early episode of intense bombardment have been largely obliterated by later volcanism, tectonism, erosion, and sedimentation by wind and water, and by circumpolar glacial and periglacial processes. South of 47˚ N. the plains are dissected by numerous channels, most of which drained off a broad volcanic upland near the southern border of the quadrangle. The impressive Elysium volcanoes cap the crest of this upland; their northernmost member, Hecates Tholus, lies within the Cebrenia quadrangle. The southeastern part of the Cebrenia quadrangle is dominated by the Phlegra Montes, which may be the only purely tectonic mountain range on Mars. It seems to have been formed by block faulting; there is no evidence that impact of volcanic processes played a role. An ancient pediment appears to have been uplifted by normal faults to form a north- to north-northeast-trending mountain range 1,400 km long, as much as 250 km wide, and more than 1 km high. Its foothills are partly covered by later volcanic and eolian deposits.

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USGS1979

Geologic map of the Phaethontis Quadrangle of Mars

The Phaethontis quadrangle of Mars is dominated by densely cratered uplands and plateaus which form some of the oldest surfaces on the planet. Extensive low-lying areas within the cratered terrains, including the floors of the large craters , are covered to different degrees by plains-forming material. The youngest plains unit surround Tharsis Montes to the north. Various erosional processes, including eolian scour and possibly scarp retreat through volatile-release sapping and mass wasting, producing several distinctive physiographic features: knob and mesa terrains, plains and small knobs, and plateaus dissected by furrows, steep walled gorges, and pits.

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